The first view of ? Scuti and ? Doradus stars with the TESS mission

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dc.authoridDaszynska-Daszkiewicz, Jadwiga/0000-0001-9704-6408
dc.authoridAntoci, Victoria/0000-0002-0865-3650
dc.authoridBorre, Camilla/0000-0003-1286-8512
dc.authoridMurphy, Simon/0000-0002-5648-3107
dc.authoridJustesen, Anders Zinck/0000-0002-0174-2466
dc.authoridMonteiro, Mario J.P.F.G./0000-0003-0513-8116
dc.authoridWeiss, Werner W./0000-0003-3977-4436
dc.contributor.authorAntoci, V.
dc.contributor.authorCunha, M. S.
dc.contributor.authorBowman, D. M.
dc.contributor.authorMurphy, S. J.
dc.contributor.authorKurtz, D. W.
dc.contributor.authorBedding, T. R.
dc.contributor.authorBorre, C. C.
dc.date.accessioned2025-01-27T20:50:17Z
dc.date.available2025-01-27T20:50:17Z
dc.date.issued2019
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractWe present the first asteroseismic results for delta Scuti and gamma Doradus stars observed in Sectors 1 and 2 of the TESS mission. We utilize the 2-min cadence TESS data for a sample of 117 stars to classify their behaviour regarding variability and place them in the Hertzsprung-Russell diagram using Gaia DR2 data. Included within our sample are the eponymous members of two pulsator classes, gamma Doradus and SX Phoenicis. Our sample of pulsating intermediate-mass stars observed by TESS also allows us to confront theoretical models of pulsation driving in the classical instability strip for the first time and show that mixing processes in the outer envelope play an important role. We derive an empirical estimate of 74 per cent for the relative amplitude suppression factor as a result of the redder TESS passband compared to the Kepler mission using a pulsating eclipsing binary system. Furthermore, our sample contains many high-frequency pulsators, allowing us to probe the frequency variability of hot young d Scuti stars, which were lacking in the Kepler mission data set, and identify promising targets for future asteroseismic modelling. The TESS data also allow us to refine the stellar parameters of SX Phoenicis, which is believed to be a blue straggler.
dc.description.sponsorshipNASA Explorer Program; Danish National Re-search Foundation [DNRF106]; ESA PRODEX [PEA 4000119301]; Stellar Astrophysics Centre (SAC) at Aarhus University; NASA [NAS5-2655]; Danish National Research Foundation [DNRF106]; FCT -Fundacao para a Ciencia e a Tecnologia; FEDER through COMPETE2020 -Programa Operacional Competitividade e Internacionalizacao [UID/FIS/04434/2019, PTDC/FIS-AST/30389/2017, POCI-01-0145-FEDER-030389]; FCT [CEECIND/02619/2017]; Polish National Science Center (NCN) [2018/29/B/ST9/02803, 2015/18/A/ST9/00578, 2016/21/B/ST9/01126]; Spanish public funds under Spanish Ministry of Science and Education [ESP201787676-2-2, ESP2015-65712-C5-5-R]; NSF REU program [PHY-1359195]; Lendulet Program of the Hungarian Academy of Sciences [LP2018-7/2018]; National Research, Development and Innovation Fund of Hungary under the K16 funding scheme [115709]; Spanish public funds [ESP2015-65712-C5-5-R, ESP2017-87676-2-2, ESP2017-87676-C5-5-R]; 'Ramon y Cajal' program of the Spanish Ministry of Science and Education [RYC2012-09913]; European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme [670519: MAMSIE]; KULeuven Research Council [C16/18/005: PARADISE]; Research Foundation Flanders (FWO) [G0H5416N]; BELgian federal Science Policy Office (BELSPO) through PRODEX grant PLATO; Spanish State Research Agency (AEI) [ESP2017-87676-C5-1-R, MDM-2017-0737]; National Research, Development and Innovation Fund of Hungary [PD-123910, PD1717]; Whitaker Foundation; Natural Sciences and Engineering Research Council of Canada; 'Programme National de Physique Stellaire' (PNPS) of CNRS/INSU - CEA; CNES; Polish NCN [2015/18/A/ST9/00578]; Postdoc@MUNI project [CZ.02.2.69/0.0/0.0/16-027/0008360]; State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award [SEV-2017-0709]; STFC [ST/N504348/1, ST/R000603/1]; DGAPA-UNAM [PAPIIT IN100918]; Ministry of Science and Technology of Thailand; French Agence Nationale de la Recherche (ANR), under grant ESRR [ANR-16-CE31-0007-01]; NSFC of China [11873084, 11521303]; YunnanApplied Basic Research Projects [2017B008]; Bulgarian NSF [DN 08-1/2016]; Fonds Wetenschappelijk Onderzoek - Vlaanderen (FWO) [G0H5416N]; National Aeronautics and Space Administration; National Science Foundation; [DN 18/13-12.12.2017]; STFC [ST/R000603/1] Funding Source: UKRI
dc.description.sponsorshipWe thank the referee for useful comments and discussions. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. Funding for the TESS Asteroseismic Science Operations Centre is provided by the Danish National Re-search Foundation (Grant agreement no.: DNRF106), ESA PRODEX (PEA 4000119301), and Stellar Astrophysics Centre (SAC) at Aarhus University. We thank the TESS and TASC/TASOC teams for their support of this work. This research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-2655. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106). MC was supported by FCT -Fundacao para a Ciencia e a Tecnologia through national funds and by FEDER through COMPETE2020 -Programa Operacional Competitividade e Internacionalizacao by these grants: UID/FIS/04434/2019, PTDC/FIS-AST/30389/2017, and POCI-01-0145-FEDER-030389. MC is supported in the form of work contract funded by national funds through FCT (CEECIND/02619/2017). JDD acknowledges support from the Polish National Science Center (NCN), grant no. 2018/29/B/ST9/02803. AGH acknowledges funding support from Spanish public funds for research under projects ESP201787676-2-2 and ESP2015-65712-C5-5-R of the Spanish Ministry of Science and Education. FKA gratefully acknowledges funding through grant 2015/18/A/ST9/00578 of the Polish National Science Centre (NCN). JPe acknowledges funding support from the NSF REU program under grant number PHY-1359195. APi and KK acknowledge support provided by the Polish National Science Center (NCN) grant No. 2016/21/B/ST9/01126. This project has been supported by the Lendulet Program of the Hungarian Academy of Sciences, project No. LP2018-7/2018, and by the support provided from the National Research, Development and Innovation Fund of Hungary, financed under the K16 funding scheme, project No. 115709. JCS acknowledges funding support from Spanish public funds for research under projects ESP2017-87676-2-2 and ESP2015-65712-C5-5-R, and from project RYC2012-09913 under the 'Ramon y Cajal' program of the Spanish Ministry of Science and Education. The research leading to these results has (partially) received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement N.670519: MAMSIE), from the KULeuven Research Council (grant C16/18/005: PARADISE), from the Research Foundation Flanders (FWO) under grant agreement G0H5416N (ERC Runner Up Project), as well as from the BELgian federal Science Policy Office (BELSPO) through PRODEX grant PLATO. SBF acknowledges support by the Spanish State Research Agency (AEI) through project No. 'ESP2017-87676-C5-1-R' and No MDM-2017-0737 Unidad de Excelencia `Maria de Maeztu'-Centro de Astrobiolog ' ia (CSICINTA). ZsB acknowledges the support provided from the National Research, Development and Innovation Fund of Hungary, financed under the PD1717 funding scheme, project no. PD-123910. DLB acknowledges support from the Whitaker Foundation. SC gratefully acknowledges funding through grant 2015/18/A/ST9/00578 of the Polish National Science Centre (NCN). CCL gratefully acknowledges support from the Natural Sciences and Engineering Research Council of Canada. GMM acknowledges funding by the STFC consolidated grant ST/R000603/1. RMO, SC, and DR were supported in this work by the 'Programme National de Physique Stellaire' (PNPS) of CNRS/INSU co-funded by CEA and CNES. IS acknowledges the partial support of projects DN 08-1/2016 and DN 18/13-12.12.2017. PS acknowledges financial support by the Polish NCN grant 2015/18/A/ST9/00578. MS acknowledges the Postdoc@MUNI project CZ.02.2.69/0.0/0.0/16-027/0008360. JPG, JRR, and MLM acknowledge funding support from Spanish public funds for research under project ESP2017-87676-C5-5-R and from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). JAE acknowledges STFC for funding support (reference ST/N504348/1). LFM acknowledges the financial support from the DGAPA-UNAM under grant PAPIIT IN100918. DMk acknowledges his work as part of the research activity of the National Astronomical Research Institute of Thailand (NARIT), which is supported by the Ministry of Science and Technology of Thailand. MR acknowledges the support of the French Agence Nationale de la Recherche (ANR), under grant ESRR (ANR-16-CE31-0007-01). We acknowledge the International Space Science Institute (ISSI) for supporting the SoFAR international team http://www.issi.unibe.ch/teams/sofar/.TW acknowledges the NSFC of China (Grant Nos. 11873084 and 11521303) and YunnanApplied Basic Research Projects (GrantNo. 2017B008). IS acknowledges for a partial support of DN 08-1/2016 funded by the Bulgarian NSF. This work hasmade use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, ht tps://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The research leading to these results has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No. 670519: MAMSIE) and from the Fonds Wetenschappelijk Onderzoek - Vlaanderen (FWO) under the grant agreement G0H5416N (ERC Opvangproject). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France (DOI: 10.26093/cds/vizier). The original description of the VizieR service was published in A&AS 143, 23. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.
dc.identifier.doi10.1093/mnras/stz2787
dc.identifier.endpage4059
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.issue3
dc.identifier.scopus2-s2.0-85079595712
dc.identifier.scopusqualityQ1
dc.identifier.startpage4040
dc.identifier.urihttps://doi.org/10.1093/mnras/stz2787
dc.identifier.urihttps://hdl.handle.net/20.500.12428/25460
dc.identifier.volume490
dc.identifier.wosWOS:000503993100070
dc.identifier.wosqualityQ1
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherOxford Univ Press
dc.relation.ispartofMonthly Notices of The Royal Astronomical Society
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/openAccess
dc.snmzKA_WoS_20250125
dc.subjectasteroseismology
dc.subjecttechniques: photometric
dc.subjectstars: chemically peculiar
dc.subjectstars: interiors
dc.subjectstars: variables: delta Scuti
dc.titleThe first view of ? Scuti and ? Doradus stars with the TESS mission
dc.typeArticle

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